The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane

Schisano, E.; Molinari, S.; Elia, D.; Benedettini, M.; Olmi, L.; Pezzuto, S.; Traficante, A.; Brescia, M.; Cavuoti, S.; Giorgio, A. M. Di; Liu, S J; Moore, T. J. T.; Noriega-Crespo, A.; Riccio, G.; Baldeschi, A.; Becciani, U.; Peretto, N.; Merello, Manuel; Vitello, F.; Zavagno, A.; Beltrán, M. T.; Cambrésy, L.; Eden, David; Causi, G. Li; Molinaro, M.; Palmeirim, P.; Sciacca, Eva; Testi, L.; Umana, G.; Whitworth, Anthony Peter

doi:10.1093/mnras/stz3466

Cited by 52 publications

(15 citation statements)

References 135 publications

(286 reference statements)

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“…The clump masses and cloud masses have been calculated using different dust opacity values. The ATLASGAL survey uses an opacity of 1.85 cm 2 g −1 at ν 0 = 350 GHz (Schuller et al 2009 and references therein) while the SEDIGISM survey uses a CO-H 2 conversion (CO X factor ∼ 1.08±0.19×10 21 cm −2 (K km s −1 ) −1 ; see Paper I for details) that is derived from the dust opacity used by the Hi-GAL column density maps (Elia et al 2013;Schisano et al 2020; κ 0 = 0.1 cm 2 g −1 at ν 0 = 1200 GHz; Hildebrand 1983). Following the reference of Elia et al (2013) the opacity is assumed to scale as:…”

Section: Dense Gas Fractionmentioning

confidence: 99%

SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc

Urquhart

Figura

Cross

et al. 2020

Monthly Notices of the Royal Astronomical Society

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By combining two surveys covering a large fraction of the molecular material in the Galactic disk we investigate the role the spiral arms play in the star formation process. We have matched clumps identified by ATLASGAL with their parental GMCs as identified by SEDIGISM, and use these giant molecular cloud (GMC) masses, the bolometric luminosities, and integrated clump masses obtained in a concurrent paper to estimate the dense gas fractions (DGFgmc = ∑Mclump/Mgmc) and the instantaneous star forming efficiencies (i.e., SFEgmc = ∑Lclump/Mgmc). We find that the molecular material associated with ATLASGAL clumps is concentrated in the spiral arms (∼60 per cent found within ±10 km s−1 of an arm). We have searched for variations in the values of these physical parameters with respect to their proximity to the spiral arms, but find no evidence for any enhancement that might be attributable to the spiral arms. The combined results from a number of similar studies based on different surveys indicate that, while spiral-arm location plays a role in cloud formation and H i to H2 conversion, the subsequent star formation processes appear to depend more on local environment effects. This leads us to conclude that the enhanced star formation activity seen towards the spiral arms is the result of source crowding rather than the consequence of a any physical process.

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Section: Dense Gas Fractionmentioning

confidence: 99%

SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc

Urquhart

Figura

Cross

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…To detect filaments in the Serpens/Aquila East data, we applied to the column density map the algorithm presented in Schisano et al (2014) and Schisano et al (2020), to which we refer the reader for a complete description of the algorithm. Here we just summarise basic details.…”

Section: Relationship Between Cores and Filamentary Structure In Serpensmentioning

confidence: 99%

“…Here we just summarise basic details. Among several definitions of filaments, given in the recent literature , the one adopted by Schisano et al (2020) is "any extended two-dimensional, cylindrical-like feature that is elongated and shows a higher brightness contrast with respect to its surroundings". Starting from this definition, such structures are identified by using the Hessian Matrix H(x, y) of an image, its eigenvalues λa, λ b , and their linear combination.…”

Section: Relationship Between Cores and Filamentary Structure In Serpensmentioning

confidence: 99%

“…This algorithm requests two input parameters: a threshold value T r and a dilation parameter, that permits to extend the initial mask (essentially based on the filament spine) in order to include the entire filament area with its borders. In Appendix B of Schisano et al (2020) the range of variability for these parameters is widely investigated, and the choice of default values for them is justified. Here we use the default value to set the dilation parameter, and T r = 3.5 × σ as threshold value, different from the default value T r = 3 × σ, because on the one hand it corresponds to a better definition and separation of filaments in the Serpens Main region (especially in Clusters A and B), and, on the other hand, it makes no appreciable changes on filaments extracted in the Aquila East region.…”

Section: Relationship Between Cores and Filamentary Structure In Serpensmentioning

confidence: 99%

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The census of dense cores in the Serpens region from the Herschel Gould Belt Survey

Fiorellino,

Elia,

André

et al. 2020

Preprint

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The Herschel Gould Belt survey mapped the nearby (d < 500 pc) star-forming regions to understand better how the prestellar phase influences the star formation process. Here we report a complete census of dense cores in a ∼ 15 deg 2 area of the Serpens star-forming region located between d ∼ 420 pc and 484 pc. The PACS and SPIRE cameras imaged this cloud from 70 µm to 500 µm. With the multi-wavelength source extraction algorithm getsources , we extract 833 sources, of which 709 are starless cores and 124 are candidate proto-stellar cores. We obtain temperatures and masses for all the sample, classifying the starless cores in 604 prestellar cores and 105 unbound cores. Our census of sources is 80% complete for M > 0.8 M overall. We produce the core mass function (CMF) and compare it with the initial mass function (IMF). The prestellar CMF is consistent with log-normal trend up to ∼ 2 M , after which it follows a power-law with slope of −2.05 ± 0.34. The tail of its CMF is steeper but still compatible with the IMF for the region we studied in this work. We also extract the filaments network of the Serpens region, finding that 81% of prestellar cores lie on filamentary structures. The spatial association between cores and filamentary structure supports the paradigm, suggested by other Herschel observations, that prestellar cores mostly form on filaments. Serpens is confirmed to be a young, low-mass and active star-forming region.

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“…While Herschel observations were focused on nearby clouds, extensive galactic-wide surveys of filamentary structures have been performed to date (e.g. Li et al 2016;Schisano et al 2020). Statistical distributions of basic physical parameters of interstellar filaments have been derived.…”

Section: Introductionmentioning

confidence: 99%

A multi-line study of the filamentary infrared dark cloud G351.78-0.54

Ryabukhina,

Zinchenko

2021

Preprint

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We present results of a multi-line study of the filamentary infrared dark cloud G351.78-0.54 in the 1.3 and 0.8 mm wavelength bands. The lines of the three isotopologues of carbon monoxide CO, N 2 H + , CH 3 CCH and HNCO were observed. The aim was to study the general structure of the filamentary cloud, its fragmentation and physical parameters with the emphasis on properties of dense clumps in this cloud. Several dense clumps are identified from the N 2 H + (3-2) data, their masses and virial parameters are determined using the C 18 O (2-1) line. Temperatures of some clumps are estimated from the CH 3 CCH and HNCO data. Almost all clumps appear to be gravitationally unstable. The density estimates obtained from the C 18 O (3-2)/(2-1) and N 2 H + (3-2)/(1-0) intensity ratios are in the range 𝑛 ∼ (0.3 − 3) × 10 5 cm −3 . The HNCO emission is detected exclusively toward the first clump which contains the luminous IR source IRAS 17233-3606, and indicates an even higher density. It is observed in the outflow, too. The velocity shift of the higher excitation HNCO lines may indicate a movement of the hot core relative the surrounding medium. In some clumps there is a velocity shift ∼ 1 km s −1 between N 2 H + (3-2) and CO isotopologues. The large widths of the N 2 H + (3-2) line in the clumps indicate an increase of the velocity dispersion in their dense interiors, which may be related to the star formation process. The N 2 H + abundance drops toward the luminous IR source.

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The Hi-GAL catalogue of dusty filamentary structures in the Galactic plane

Cited by 52 publications

References 135 publications

SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc

SEDIGISM-ATLASGAL: dense gas fraction and star formation efficiency across the Galactic disc

The census of dense cores in the Serpens region from the Herschel Gould Belt Survey

A multi-line study of the filamentary infrared dark cloud G351.78-0.54

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